glossary - Discovery Education
... nebula and a white dwarf. parsec — a distance of 3.26 light-years; used to measure immense distances in space. planetary nebula — a ring of dust and gas blown off a red giant star after it undergoes an explosion. pulsar — a rapidly spinning neutron star that sends out pulses of radiation at regular ...
... nebula and a white dwarf. parsec — a distance of 3.26 light-years; used to measure immense distances in space. planetary nebula — a ring of dust and gas blown off a red giant star after it undergoes an explosion. pulsar — a rapidly spinning neutron star that sends out pulses of radiation at regular ...
Life Cycle of Stars
... 1) Once your teacher has approved each word timeline and you have recorded them on the back of this page, you will create a large poster that visually displays the four life cycles. 2) Use your notes, RQs, video notes and a computer or phone to complete the following: a) Name of star stage b) Color ...
... 1) Once your teacher has approved each word timeline and you have recorded them on the back of this page, you will create a large poster that visually displays the four life cycles. 2) Use your notes, RQs, video notes and a computer or phone to complete the following: a) Name of star stage b) Color ...
Life Cycle of Stars - Lab Science Schedule
... depends on the mass of the star when it was first formed. The smaller the starting mass of a star, the longer it will live. IV. Massive Stars When massive stars are formed, they usually have at least six times as much mass as the sun. Massive stars start out like medium sized stars and continue on t ...
... depends on the mass of the star when it was first formed. The smaller the starting mass of a star, the longer it will live. IV. Massive Stars When massive stars are formed, they usually have at least six times as much mass as the sun. Massive stars start out like medium sized stars and continue on t ...
ASTR2050 Spring 2005 •
... Example: How long would the Sun live if its energy was from gravitational collapse? Answer: Estimate available energy from gravitation and use the known luminosity to get a time ...
... Example: How long would the Sun live if its energy was from gravitational collapse? Answer: Estimate available energy from gravitation and use the known luminosity to get a time ...
Introduction to Astrophysics Tutorial 4: Supernovae
... A second channel for stellar explosions involves an accreting white dwarf. When it approached MCh (but before actually reaching it), its C is ignited. Because of the high degeneracy (i.e. pressure weakly depends on temperature), the fusion process is a runaway one, burning the entire white dwarf, an ...
... A second channel for stellar explosions involves an accreting white dwarf. When it approached MCh (but before actually reaching it), its C is ignited. Because of the high degeneracy (i.e. pressure weakly depends on temperature), the fusion process is a runaway one, burning the entire white dwarf, an ...
characteristics of stars/lives of stars
... 5. What are the main characteristics used to classify stars? ...
... 5. What are the main characteristics used to classify stars? ...
Galaxies and Stars Questions KEY
... Generally, stars with more mass have shorter life spans because they burn their fuel more quickly than smaller stars do. The mass also determines which direction the lifespan goes and ultimately, determines what the star becomes when it dies. 7. What is the outcome of a star that runs out of hydroge ...
... Generally, stars with more mass have shorter life spans because they burn their fuel more quickly than smaller stars do. The mass also determines which direction the lifespan goes and ultimately, determines what the star becomes when it dies. 7. What is the outcome of a star that runs out of hydroge ...
Facts - GreenSpirit
... In the middle of these condensation points, pressure of the gases build producing heat ...
... In the middle of these condensation points, pressure of the gases build producing heat ...
ppt - Slides by Prof Christian
... (low mass) are the most common stars. Bright, hot, blue main-sequence stars (highmass) are very rare. Giants and supergiants are extremely rare. ...
... (low mass) are the most common stars. Bright, hot, blue main-sequence stars (highmass) are very rare. Giants and supergiants are extremely rare. ...
CBradleyLoutl
... . Most of a star is hydrogen, less than a quarter is helium, maybe 1 part per thousand will be heavier elements. . Looking at what wavelengths of light are present on emission/absorption spectra will tell exact constituents. Examples: ...
... . Most of a star is hydrogen, less than a quarter is helium, maybe 1 part per thousand will be heavier elements. . Looking at what wavelengths of light are present on emission/absorption spectra will tell exact constituents. Examples: ...
Abstract Submitted for the PHY599 Meeting of
... age is that it allows the study of the time evolution of astronomical phenomena related to stars and their surrounding bodies. I will start with a basic and short description of the Hertzsprung-Russell-Diagram, which allows (together with stellar evolutionary models) an age determination for star cl ...
... age is that it allows the study of the time evolution of astronomical phenomena related to stars and their surrounding bodies. I will start with a basic and short description of the Hertzsprung-Russell-Diagram, which allows (together with stellar evolutionary models) an age determination for star cl ...
The Hidden Lives of Galaxies NSTA 2001
... This presentation, and other materials on the Life Cycles of Stars, are available on the Imagine the Universe! web site at: http://imagine.gsfc.nasa.gov/docs/teachers/lifecycles/stars.html ...
... This presentation, and other materials on the Life Cycles of Stars, are available on the Imagine the Universe! web site at: http://imagine.gsfc.nasa.gov/docs/teachers/lifecycles/stars.html ...
M What is the emptiness before the Big Bang? R Read the variables
... What type of galaxy is this? What is the name of this graph that demosntrates the postive relationship between a star’s temperature and brightness? ...
... What type of galaxy is this? What is the name of this graph that demosntrates the postive relationship between a star’s temperature and brightness? ...
Properties of stars during hydrogen burning
... Energy transport to the surface - cooling: The star will settle into a hydrostatic and thermal equilibrium, where cooling is balanced by nuclear energy generation and there is no time dependence of any state variables. The generated heat will then exactly match the outgoing energy flow (luminosity) ...
... Energy transport to the surface - cooling: The star will settle into a hydrostatic and thermal equilibrium, where cooling is balanced by nuclear energy generation and there is no time dependence of any state variables. The generated heat will then exactly match the outgoing energy flow (luminosity) ...
Science Olympiad - Department of Physics and Astronomy
... relationship between period and luminosity or absolute magnitude. This absolute magnitude can be calculated as a function of the variable’s period. Comparing this to its apparent magnitude one can calculate the distance with the ...
... relationship between period and luminosity or absolute magnitude. This absolute magnitude can be calculated as a function of the variable’s period. Comparing this to its apparent magnitude one can calculate the distance with the ...
Notes: Star Formation
... • Brown Dwarfs don’t get hot enough to start fusion. • They shine dimly, but slowly cool off. ...
... • Brown Dwarfs don’t get hot enough to start fusion. • They shine dimly, but slowly cool off. ...
Science Olympiad - UNC Physics and Astronomy
... 700 million tons of hydrogen are converted to helium each second ...
... 700 million tons of hydrogen are converted to helium each second ...
Star Cycle Notes
... Star Cycle Notes Stars begin their life as collections of gas and dust called stellar nebulas. These nebulas condense and become more massive. Once gravity exerts enough pressure on the core, nuclear fusion begins fusing hydrogen atoms together to form helium, and releases a tremendous amount of ene ...
... Star Cycle Notes Stars begin their life as collections of gas and dust called stellar nebulas. These nebulas condense and become more massive. Once gravity exerts enough pressure on the core, nuclear fusion begins fusing hydrogen atoms together to form helium, and releases a tremendous amount of ene ...
here
... 1: Red dwarf (e.g., an M star) implies low-mass. Low-metallicity implies Pop II. Perpendicular through the disk implies not a disk-like orbit. Thus, this is likely an old, Pop II star from the stellar halo of the Milky Way. 2: Before Big Bang Nucleosynthesis, the universe was too hot for nuclei like ...
... 1: Red dwarf (e.g., an M star) implies low-mass. Low-metallicity implies Pop II. Perpendicular through the disk implies not a disk-like orbit. Thus, this is likely an old, Pop II star from the stellar halo of the Milky Way. 2: Before Big Bang Nucleosynthesis, the universe was too hot for nuclei like ...
STARS
... layers by radiation and convection •May take millions of years for energy to work its way through star to surface ...
... layers by radiation and convection •May take millions of years for energy to work its way through star to surface ...
Ch. 14 Formation of Stars
... • Stars that are lighter than 0.4 suns have relatively cool interiors, which makes them more opaque to photons. • As a result, radiation cannot easily flow through any part of them, so they only have convective zones. No radiative zones. • Core convective zone • “Stars” between 0.08 and 0.012 sola ...
... • Stars that are lighter than 0.4 suns have relatively cool interiors, which makes them more opaque to photons. • As a result, radiation cannot easily flow through any part of them, so they only have convective zones. No radiative zones. • Core convective zone • “Stars” between 0.08 and 0.012 sola ...
Stellar Evolution Reading Questions Integrated Science 2 Name
... shock wave from an ___________________ of a nearby star may trigger the contraction. Once the process begins, _________________ squeezes particles in the nebula, pulling every particle toward the _____________. As the nebula shrinks, gravitational energy is converted to _______________ energy. 3. Mo ...
... shock wave from an ___________________ of a nearby star may trigger the contraction. Once the process begins, _________________ squeezes particles in the nebula, pulling every particle toward the _____________. As the nebula shrinks, gravitational energy is converted to _______________ energy. 3. Mo ...
Main sequence
In astronomy, the main sequence is a continuous and distinctive band of stars that appears on plots of stellar color versus brightness. These color-magnitude plots are known as Hertzsprung–Russell diagrams after their co-developers, Ejnar Hertzsprung and Henry Norris Russell. Stars on this band are known as main-sequence stars or ""dwarf"" stars.After a star has formed, it generates thermal energy in the dense core region through the nuclear fusion of hydrogen atoms into helium. During this stage of the star's lifetime, it is located along the main sequence at a position determined primarily by its mass, but also based upon its chemical composition and other factors. All main-sequence stars are in hydrostatic equilibrium, where outward thermal pressure from the hot core is balanced by the inward pressure of gravitational collapse from the overlying layers. The strong dependence of the rate of energy generation in the core on the temperature and pressure helps to sustain this balance. Energy generated at the core makes its way to the surface and is radiated away at the photosphere. The energy is carried by either radiation or convection, with the latter occurring in regions with steeper temperature gradients, higher opacity or both.The main sequence is sometimes divided into upper and lower parts, based on the dominant process that a star uses to generate energy. Stars below about 1.5 times the mass of the Sun (or 1.5 solar masses (M☉)) primarily fuse hydrogen atoms together in a series of stages to form helium, a sequence called the proton–proton chain. Above this mass, in the upper main sequence, the nuclear fusion process mainly uses atoms of carbon, nitrogen and oxygen as intermediaries in the CNO cycle that produces helium from hydrogen atoms. Main-sequence stars with more than two solar masses undergo convection in their core regions, which acts to stir up the newly created helium and maintain the proportion of fuel needed for fusion to occur. Below this mass, stars have cores that are entirely radiative with convective zones near the surface. With decreasing stellar mass, the proportion of the star forming a convective envelope steadily increases, whereas main-sequence stars below 0.4 M☉ undergo convection throughout their mass. When core convection does not occur, a helium-rich core develops surrounded by an outer layer of hydrogen.In general, the more massive a star is, the shorter its lifespan on the main sequence. After the hydrogen fuel at the core has been consumed, the star evolves away from the main sequence on the HR diagram. The behavior of a star now depends on its mass, with stars below 0.23 M☉ becoming white dwarfs directly, whereas stars with up to ten solar masses pass through a red giant stage. More massive stars can explode as a supernova, or collapse directly into a black hole.